Densities of the three constituent spheroids of the same eccentricity as our earlier model of the Galaxy are assumed to be given by an analytical form of ρ i (r)= k i e − m i r u i , where k i , m i , and α i are obtained by comparing with the results of the previous model. Using three values of ρ i (r) the galactic rotation curve, mass of each spheroid and the whole Galaxy are calculated, and the three dimensional density distribution in the Galaxy is also obtained. The calculated rotation curve of the model Galaxy is in good agreement with the observed curve, and the shape of the cross section of the model Galaxy given by the computed density is very similar to the inferred shape of the spiral galaxies.

An improved version of the galatic mass distribution has been derived by increasing the number of shells in each spheroid of our earlier model. It is found that the increase of the number of the shell improves the model considerably, thus making it agree far better with observations.

The position and magnitude of 1449 stars listed in "Seoung Kyung" (by Byung Kil Nahm, 1861) are compared with those in modern western star catalogues for their identification. 923 stars out of 1449 stars were identified within the range of accuracy. Δ α ≤ 20 s .0 , Δ δ ≤ 1 ′ .0 a n d Δ m = 0 o r ± 1 . When Δ α a n d Δ δ increased to Δ α ≤ 1 m . 0 , Δ δ ≤ 15 ′ .0 a n d Δ m = 0 or +1, 399 more stars could be included in the list.

A simple model of the galactic mass distribution consisting of one sphere and two spheroids with different eccentricities is considered. The resulting model is found to be consistent with the recent observations of the galactic rotation as well as suggested shape of the Galaxy.

The average velocity, 330km/sec. of the high velocity stars with respect to the galactic center is obtained from the data used by Fricke on the assumption that the rotational velocity of the Local Standard of Rest is 250km/sec. Comparing this value with the escape velocity, 380km/sec, at the solar neighborhood which is calculated from Mestel's model of the Galaxy, it is shown that most of the high velocity stars are bound to the Galaxy and that their average apogalacticon is about 40 kpc from the galactic center. And the fact that stars with radial velocities larger than 63km/sec are missing in the direction of galactic rotation of L.S.R. is interpreted as the result partly of the random distribution of the directions of motion of the high velocity stars and partly of the observational errors.

Optical thickness of Rosette Nebula for Lyman Continuum is examined with W. Gebel's data. And the effective temperatures of the six exciting 0 stars of the nebula are obtained on the assumption that O stars emit black body radiation. The results are found to be generally in between Spitzers old and revised values.

By comparison and analysis of the optical data of the two galactic clusters of Pleiades and h and x Persei and the radio data of the HI gas clouds which are related with those two clusters, the relative motions of those gas clouds with retpect to the two clusters were obtained. The three theories on the acceleration of HI gas cloud surrounding a star cluster by Blaauw. Oort and Spitzer, and Kahn were examined with the above obtained kinetic data of the Pleiades and the h and x Penei clouds. And it was shown that Blaauw's theory is applicable to the h and x Persoi clouds but not to the Pleiades, that Dart and Spitzer's theory can explain the motions of both clouds, and that Kahn's theory needs more improvement to be a complete one.